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Infrared Experiments for Spaceborne Planetary Atmospheres Research Full Report
NASA Technical Memorandum 84414 Infrared Experiments for Spaceborne Planetary Atmospheres Research Full Report Infrared Experiments Working Group NOVEMBER 1981 NASA NASA Technical Memorandum 84414 Infrared Experiments for Spaceborne Planetary Atmospheres Research Full Report Infrared Experiments Working Group Jet Propulsion Laboratory Pasadena, California NASA National Aeronautics and Space Administration Scientific and Technical Information Branch 1981 TABLE OF CONTENTS Preface Summary of Principal Conclusions and Recommendations Chapter I The Role of Infrared Sensing in Atmospheric Science Chapter II Review of Existing Infrared Measurement Techniques Chapter III Critical Comparison of Proposed Measurement Techniques Chapter IV Conclusions and Recommended Instrument Developments Appendices: A Critical Technologies B Applicability of Atmospheric Infrared Instrumentation to Surface Science C Supporting Studies in Data Analysis and Numerical Modeling D Description of Planned Earth Orbital Platforms ii PREFACE Experiments conducted in the infrared spectral region provide a powerful tool for the study of the composition, structure and dynamics of planetary atmospheres. However, the field has become highly complex, especially that part associated with spacecraft sensing, and the range of technologies used so diverse that it is difficult to determine which of the available methods for making a particular measurement is to be preferred, even for those deeply involved in the field. Unfortunately, the realities of the age demand that some selectivity be employed; not all approaches can be supported. Furthermore, the chosen methods are generally sufficiently untried that long pre-flight developments are neces- sary if viable proposals are to be written for future flight opportunities. These considerations clearly lead to a program of developments which must be coordinated on a national scale. -
EDL – Lessons Learned and Recommendations
."#!(*"# 0 1(%"##" !)"#!(*"#* 0 1"!#"("#"#(-$" ."!##("""*#!#$*#( "" !#!#0 1%"#"! /!##"*!###"#" #"#!$#!##!("""-"!"##&!%%!%&# $!!# %"##"*!%#'##(#!"##"#!$$# /25-!&""$!)# %"##!""*&""#!$#$! !$# $##"##%#(# ! "#"-! *#"!,021 ""# !"$!+031 !" )!%+041 #!( !"!# #$!"+051 # #$! !%#-" $##"!#""#$#$! %"##"#!#(- IPPW Enabled International Collaborations in EDL – Lessons Learned and Recommendations: Ethiraj Venkatapathy1, Chief Technologist, Entry Systems and Technology Division, NASA ARC, 2 Ali Gülhan , Department Head, Supersonic and Hypersonic Technologies Department, DLR, Cologne, and Michelle Munk3, Principal Technologist, EDL, Space Technology Mission Directorate, NASA. 1 NASA Ames Research Center, Moffett Field, CA [email protected]. 2 Deutsches Zentrum für Luft- und Raumfahrt e.V. (DLR), German Aerospace Center, [email protected] 3 NASA Langley Research Center, Hampron, VA. [email protected] Abstract of the Proposed Talk: One of the goals of IPPW has been to bring about international collaboration. Establishing collaboration, especially in the area of EDL, can present numerous frustrating challenges. IPPW presents opportunities to present advances in various technology areas. It allows for opportunity for general discussion. Evaluating collaboration potential requires open dialogue as to the needs of the parties and what critical capabilities each party possesses. Understanding opportunities for collaboration as well as the rules and regulations that govern collaboration are essential. The authors of this proposed talk have explored and established collaboration in multiple areas of interest to IPPW community. The authors will present examples that illustrate the motivations for the partnership, our common goals, and the unique capabilities of each party. The first example involves earth entry of a large asteroid and break-up. NASA Ames is leading an effort for the agency to assess and estimate the threat posed by large asteroids under the Asteroid Threat Assessment Project (ATAP). -
Mariner to Mercury, Venus and Mars
NASA Facts National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, CA 91109 Mariner to Mercury, Venus and Mars Between 1962 and late 1973, NASA’s Jet carry a host of scientific instruments. Some of the Propulsion Laboratory designed and built 10 space- instruments, such as cameras, would need to be point- craft named Mariner to explore the inner solar system ed at the target body it was studying. Other instru- -- visiting the planets Venus, Mars and Mercury for ments were non-directional and studied phenomena the first time, and returning to Venus and Mars for such as magnetic fields and charged particles. JPL additional close observations. The final mission in the engineers proposed to make the Mariners “three-axis- series, Mariner 10, flew past Venus before going on to stabilized,” meaning that unlike other space probes encounter Mercury, after which it returned to Mercury they would not spin. for a total of three flybys. The next-to-last, Mariner Each of the Mariner projects was designed to have 9, became the first ever to orbit another planet when two spacecraft launched on separate rockets, in case it rached Mars for about a year of mapping and mea- of difficulties with the nearly untried launch vehicles. surement. Mariner 1, Mariner 3, and Mariner 8 were in fact lost The Mariners were all relatively small robotic during launch, but their backups were successful. No explorers, each launched on an Atlas rocket with Mariners were lost in later flight to their destination either an Agena or Centaur upper-stage booster, and planets or before completing their scientific missions. -
The Pancam Instrument for the Exomars Rover
ASTROBIOLOGY ExoMars Rover Mission Volume 17, Numbers 6 and 7, 2017 Mary Ann Liebert, Inc. DOI: 10.1089/ast.2016.1548 The PanCam Instrument for the ExoMars Rover A.J. Coates,1,2 R. Jaumann,3 A.D. Griffiths,1,2 C.E. Leff,1,2 N. Schmitz,3 J.-L. Josset,4 G. Paar,5 M. Gunn,6 E. Hauber,3 C.R. Cousins,7 R.E. Cross,6 P. Grindrod,2,8 J.C. Bridges,9 M. Balme,10 S. Gupta,11 I.A. Crawford,2,8 P. Irwin,12 R. Stabbins,1,2 D. Tirsch,3 J.L. Vago,13 T. Theodorou,1,2 M. Caballo-Perucha,5 G.R. Osinski,14 and the PanCam Team Abstract The scientific objectives of the ExoMars rover are designed to answer several key questions in the search for life on Mars. In particular, the unique subsurface drill will address some of these, such as the possible existence and stability of subsurface organics. PanCam will establish the surface geological and morphological context for the mission, working in collaboration with other context instruments. Here, we describe the PanCam scientific objectives in geology, atmospheric science, and 3-D vision. We discuss the design of PanCam, which includes a stereo pair of Wide Angle Cameras (WACs), each of which has an 11-position filter wheel and a High Resolution Camera (HRC) for high-resolution investigations of rock texture at a distance. The cameras and electronics are housed in an optical bench that provides the mechanical interface to the rover mast and a planetary protection barrier. -
18Th EANA Conference European Astrobiology Network Association
18th EANA Conference European Astrobiology Network Association Abstract book 24-28 September 2018 Freie Universität Berlin, Germany Sponsors: Detectability of biosignatures in martian sedimentary systems A. H. Stevens1, A. McDonald2, and C. S. Cockell1 (1) UK Centre for Astrobiology, University of Edinburgh, UK ([email protected]) (2) Bioimaging Facility, School of Engineering, University of Edinburgh, UK Presentation: Tuesday 12:45-13:00 Session: Traces of life, biosignatures, life detection Abstract: Some of the most promising potential sampling sites for astrobiology are the numerous sedimentary areas on Mars such as those explored by MSL. As sedimentary systems have a high relative likelihood to have been habitable in the past and are known on Earth to preserve biosignatures well, the remains of martian sedimentary systems are an attractive target for exploration, for example by sample return caching rovers [1]. To learn how best to look for evidence of life in these environments, we must carefully understand their context. While recent measurements have raised the upper limit for organic carbon measured in martian sediments [2], our exploration to date shows no evidence for a terrestrial-like biosphere on Mars. We used an analogue of a martian mudstone (Y-Mars[3]) to investigate how best to look for biosignatures in martian sedimentary environments. The mudstone was inoculated with a relevant microbial community and cultured over several months under martian conditions to select for the most Mars-relevant microbes. We sequenced the microbial community over a number of transfers to try and understand what types microbes might be expected to exist in these environments and assess whether they might leave behind any specific biosignatures. -
Raman Spectroscopy of Shocked Gypsum from a Meteorite Impact Crater
International Journal of Astrobiology 16 (3): 286–292 (2017) doi:10.1017/S1473550416000367 © Cambridge University Press 2016 This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited. Raman spectroscopy of shocked gypsum from a meteorite impact crater Connor Brolly, John Parnell and Stephen Bowden Department of Geology & Petroleum Geology, University of Aberdeen, Meston Building, Aberdeen, UK e-mail: c.brolly@ abdn.ac.uk Abstract: Impact craters and associated hydrothermal systems are regarded as sites within which life could originate onEarth,and onMars.The Haughtonimpactcrater,one ofthemost well preservedcratersonEarth,is abundant in Ca-sulphates. Selenite, a transparent form of gypsum, has been colonized by viable cyanobacteria. Basementrocks, which havebeenshocked,aremoreabundantinendolithicorganisms,whencomparedwithun- shocked basement. We infer that selenitic and shocked gypsum are more suitable for microbial colonization and have enhanced habitability. This is analogous to many Martian craters, such as Gale Crater, which has sulphate deposits in a central layered mound, thought to be formed by post-impact hydrothermal springs. In preparation for the 2020 ExoMars mission, experiments were conducted to determine whether Raman spectroscopy can distinguish between gypsum with different degrees of habitability. Ca-sulphates were analysed using Raman spectroscopyand resultsshow nosignificant statistical difference between gypsumthat has experienced shock by meteorite impact and gypsum, which has been dissolved and re-precipitated as an evaporitic crust. Raman spectroscopy is able to distinguish between selenite and unaltered gypsum. This showsthat Raman spectroscopy can identify more habitable forms of gypsum, and demonstrates the current capabilities of Raman spectroscopy for the interpretation of gypsum habitability. -
Complete List of Contents
Complete List of Contents Volume 1 Cape Canaveral and the Kennedy Space Center ......213 Publisher’s Note ......................................................... vii Chandra X-Ray Observatory ....................................223 Introduction ................................................................. ix Clementine Mission to the Moon .............................229 Preface to the Third Edition ..................................... xiii Commercial Crewed vehicles ..................................235 Contributors ............................................................. xvii Compton Gamma Ray Observatory .........................240 List of Abbreviations ................................................. xxi Cooperation in Space: U.S. and Russian .................247 Complete List of Contents .................................... xxxiii Dawn Mission ..........................................................254 Deep Impact .............................................................259 Air Traffic Control Satellites ........................................1 Deep Space Network ................................................264 Amateur Radio Satellites .............................................6 Delta Launch Vehicles .............................................271 Ames Research Center ...............................................12 Dynamics Explorers .................................................279 Ansari X Prize ............................................................19 Early-Warning Satellites ..........................................284 -
Final Report Venus Exploration Targets Workshop May 19–21
Final Report Venus Exploration Targets Workshop May 19–21, 2014, Lunar and Planetary Institute, Houston, TX Conveners: Virgil (Buck) Sharpton, Larry Esposito, Christophe Sotin Breakout Group Leads Science from the Surface Larry Esposito, Univ. Colorado Science from the Atmosphere Kevin McGouldrick, Univ. Colorado Science from Orbit Lori Glaze, GSFC Science Organizing Committee: Ben Bussey, Martha Gilmore, Lori Glaze, Robert Herrick, Stephanie Johnston, Christopher Lee, Kevin McGouldrick Vision: The intent of this “living” document is to identify scientifically important Venus targets, as the knowledge base for this planet progresses, and to develop a target database (i.e., scientific significance, priority, description, coordinates, etc.) that could serve as reference for future missions to Venus. This document will be posted in the VEXAG website (http://www.lpi.usra.edu/vexag/), and it will be revised after the completion of each Venus Exploration Targets Workshop. The point of contact for this document is the current VEXAG Chair listed at ABOUT US on the VEXAG website. Venus Exploration Targets Workshop Report 1 Contents Overview ....................................................................................................................................................... 2 1. Science on the Surface .............................................................................................................................. 3 2. Science within the Atmosphere ............................................................................................................... -
Galileo in 1610
Module 3 – Nautical Science Unit 4 – Astronomy Chapter 15 - The Planets Section 2 – Mars & Jupiter What You Will Learn to Do Demonstrate understanding of astronomy and how it pertains to our solar system and its related bodies: Moon, Sun, stars and planets Objectives 1. Describe the major features of Mars 2. Identify the principal characteristics of Jupiter Key Terms CPS Key Term Questions 1 - 5 Key Terms Nix Olympica - Snow of Olympus Galilean satellites - The four largest and brightest moons of Jupiter: Io, Europa, Ganymede and Callisto; discovered by Galileo in 1610 Prograde The counter-clockwise direction of motion - celestial bodies around the Sun as seen from above the north pole of the Sun; in the sky it is from west to east Key Terms Retrograde The clockwise direction of celestial motion - bodies around the Sun; in the sky it is from east to west Rotational axis - The straight line through all fixed points of a rotating rigid body around which all other points of the body move in circles Opening Question Discuss what types of exploration missions have occurred on Mars. (Use CPS “Pick a Student” for this question.) Mars Fourth from Mars the Sun and the next planet beyond Earth, Mars has aroused the greatest interest. Mars Mars Ares (Roman Mars) Mars Named for the Roman god of war, it is often called the “red planet.” Mars Mars’ red color and its rapid movement from west to east among the stars make it stand out in the sky. Mars Earth The best time to see Mars is when it is nearest to Earth in August and September, when the Earth is Sun between the Sun and Mars. -
Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave
PROCEEDINGS OF SPIE Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave Makenzie Lystrup Howard A. MacEwen Giovanni G. Fazio Editors 10–15 June 2018 Austin, Texas, United States Sponsored by 4D Technology (United States) • Andor Technology, Ltd. (United Kingdom) • Astronomical Consultants & Equipment, Inc. (United States) • Giant Magellan Telescope (Chile) • GPixel, Inc. (China) • Harris Corporation (United States) • Materion Corporation (United States) • Optimax Systems, Inc. (United States) • Princeton Infrared Technologies (United States) • Symétrie (France) Teledyne Technologies, Inc. (United States) • Thirty Meter Telescope (United States) •SPIE Cooperating Organizations European Space Organisation • National Radio Astronomy Observatory (United States) • Science & Technology Facilities Council (United Kingdom) • Canadian Astronomical Society (Canada) Canadian Space Association ASC (Canada) • Royal Astronomical Society (United Kingdom) Association of Universities for Research in Astronomy (United States) • American Astronomical Society (United States) • Australian Astronomical Observatory (Australia) • European Astronomical Society (Switzerland) Published by SPIE Volume 10698 Part One of Three Parts Proceedings of SPIE 0277-786X, V. 10698 SPIE is an international society advancing an interdisciplinary approach to the science and application of light. The papers in this volume were part of the technical conference cited on the cover and title page. Papers were selected and subject to review by the editors and conference program committee. Some conference presentations may not be available for publication. Additional papers and presentation recordings may be available online in the SPIE Digital Library at SPIEDigitalLibrary.org. The papers reflect the work and thoughts of the authors and are published herein as submitted. The publisher is not responsible for the validity of the information or for any outcomes resulting from reliance thereon. -
Lunar and Planetary Information Bulletin, Issue
Jet Propulsion Laboratory: Where Planetary Exploration Began Note from the Editors: This issue’s lead article is the seventh in a series of reports describing the history and current activities of the planetary research facilities funded by NASA and located nationwide. This issue features the Jet Propulsion Laboratory (JPL), which since before World War II has been a leading engineering research and development center, creating America’s first satellite and most of its lunar and planetary spacecraft. It is now a major NASA center, focusing on robotic space exploration. While JPL is also very active in Earth observation and space technology programs, this article focuses on JPL’s planetary efforts. — Paul Schenk and Renee Dotson LFrom the roar of pioneering Space Age rockets to the soft whir of servos on twenty-first-century robot explorers on Mars, spacecraft designed and built at NASA’s Jet Propulsion Laboratory (JPL) have blazed the trail to the planets and into the universe beyond for nearly 60 years. The United States (U.S.) first entered space with the 1958 launch of the satellite Explorer 1, built and controlled by JPL. From orbit, Explorer 1’s voyage yielded immediate scientific results — the discovery of the Van Allen radiation belts — and led to the creation of NASA. Innovative technology from JPL has taken humanity far beyond regions of space where we can actually travel ourselves. The most distant human-made objects, Voyagers 1 and 2, were built at and are operated by JPL. From JPL’s labs and clean rooms come telescopes and cameras that have extended our vision to unprecedented depths and distances, Ppeering into the hearts of galactic clouds where new stars and planets are born, and even toward the beginning of time at the edge of the universe. -
Digital Processing of the Mariner 6 and 7 Pictures
VOL. 76, NO. 2 JOURNAL OF GEOPHYSICAL RESEARCH JANUARY 10, 1971 Digital Processing of the Mariner 6 and 7 Pictures T. C. RINDFLEISC H, J. A. DUNNE, H. ,J. FRIEDEN, W. D. STHOMBEHa, AND R. M. RUIZ Space Sciences D-ivision, J et Propttls'ion Laboratory Pasaaena, California 91103 The Mariner Mars 1969 t.elevision camera system was a vidicon-based digital system and in cluded a complex on-board video encoding and recording scheme. The spacecraft video processing was designed to maximize the volume of data returned and the encoded discriminability of the low-contrast surface detail of Mars. The ground-based photometric reconstruction of the Mariner photographs, as well as the correction of inherent vidicon camera distortion effects necessary to achieve television experiment objectives, required use of a digit.al computer to process the pictllres. The digital techniques developed to reconstl"Uct the spacecraft encoder effects and to correct for camera distortions are described and examples shown of the processed results. Specific distortion corrections that are considered include the removal of structured system noises, the removal of sensor residual image, the correction of photometric sensitivity nonunifonnit,ies and nonlinearities, the correction of geometric distortions, and the correctrn of modulat,ion transfer limitations. As all physically realizable instruments in_/ and interpretations of the imagery can be based fluence the data they collect, the Mariner Mars on information as representative of the Martian 1969 television cameras left their signatures on surface as possible. the imagery they returned to earth. Analyses The succeeding sections will describe, from of the Mariner photographs must be performed the point of view of image processing, the per with the knowledge that Mars was observed formance characteristics of the vidicon cameras through the spacecraft cameras, and any distor- and data-encoding electronics on board the tions introduced by the camera system processes spacecraft, the over-all flow of the various potentially affect the results.